Webster Cash University of Colorado X-ray Interferometry
Collaborators Ann Shipley, Karen Doty, Randy McEntaffer, & Steve Osterman at CU Nick White Goddard Marshall Joy Marshall David Windt and Steve Kahn - Columbia Mark Schattenburg - MIT Dennis Gallagher Ball Aerospace
X-ray Telescopes X-ray telescopes are sensitive to material at millions of degrees.
Capella 0.1
Capella 0.01
Capella 0.001
Capella 0.0001
Capella 0.00001
Capella 0.000001
AR Lac Simulation @ 100µas
AGN Accretion Disk Simulations @ 0.1µas C. Reynolds, U. Colorado M. Calvani, U. Padua
Need Resolution and Signal If we are going to do this, we need to support two basic capabilities: Signal Resolution
X-ray Sources Are Super Bright Example: Mass Transfer Binary 10 37 ergs/s from 10 9 cm object That is ~10,000L from 10-4 A = 10 8 B where B is the solar brightness in ergs/cm 2 /s/steradian Brightness is a conserved quantity and is the measure of visibility for a resolved object Note: Optically thin x-ray sources can have very low brightness and are inappropriate targets for interferometry. Same is true in all parts of spectrum!
Minimum Resolution
Status of X-ray Optics Modest Resolution 0.5 arcsec telescopes 0.5 micron microscopes Severe Scatter Problem Mid-Frequency Ripple Extreme Cost Millions of Dollars Each Years to Fabricate
Classes of X-ray Interferometers Dispersive Elements are Crystals or Gratings Non-Dispersive Elements are Mirrors & Telescopes
Achieving High Resolution Use Interferometry to Bypass Diffraction Limit Michelson Stellar Interferometer R=λ/20000D R in Arcsec λ in Angstroms D in Meters
Creating Fringes Requirements Path Lengths Nearly Equal Plate Scale Matched to Detector Pixels Adequate Stability Adequate Pointing Diffraction Limited Optics D d
A1 Pathlength Tolerance Analysis at Grazing Incidence A2 δ B1 = sinθ B 2 = B1cos( 2θ ) θ OPD [ 1 cos( 2θ )] sinθ δ = B1 B2 = = 2 δ sin θ θ Β1 θ Β2 A1 & A2 in Phase Here If OPD to be < λ/10 then δ < λ 20sin θ θ S1 δ S2 C d( Baseline) d( focal) < < 20sin λ λ θ 2 20sin θ cos θ
A Simple X-ray Interferometer Flats Beams Cross Detector
Wavefront Interference λ=θs (where s is fringe spacing) s s = L d λ θ=d/l
Each Mirror Was Adjustable From Outside Vacuum System was covered by thermal shroud Optics
Stray Light Facility MSFC Source, filter and slit Interferometer CCD 16m 100m Used Long Distance To Maximize Fringe Spacing
CCD Image @ 1.25keV 2 Beams Separate 2 Beams Superimposed
Fringes at 1.25keV Profile Across Illuminated Region
Test Chamber at CU Ten Meter Long Vacuum Chamber for Testing Came on-line early May EUV results good Upgrade to x-ray next
Image of Slit Reconstructed from 4 azimuths Actual Image at 30.4nm
MAXIM The Micro Arcsecond X-ray Imaging Mission Webster Cash Nicholas White Marshall Joy Colorado Goddard Marshall PLUS Contributions from the Maxim Team http://maxim.gsfc.nasa.gov
Goal Maxim: A Few Science Goals Resolve the winds of OB stars: Resolve pre-main sequence stars: Imageof center of Milky Way: Detailed images of LMC, SMC, M31: Image jets, outflows and BLR from AGN: Detailed view of starbursts: Map center of cooling flows in clusters: Detailed maps of clusters at high redshift: Image Event Horizons in AGNS: What kind of shocks drive the x ray emission? How does coronal activity interact with disk? Detect and resolve accretion disk? Supernova morphology and star formation in other settings Follow jet structure, search for scattered emission from BLR Resolve supernovae and outflows Resolve star formation regions? Cluster evolution, cooling flows Probe Extreme Gravity Limit
Flats Held in Phase Sample Many Frequencies
As More Flats Are Used Pattern Approaches Image 2 4 8 12 16 32
rces in the same e source that is displaced to the lower left. The image on the right shows 9000 total events for ity of the higher energy source. Even though the higher energy source is in the first maxima of the other, the two can still be easily distinguished.
Clockwise from upper left: Probability distribution; 100 photons randomly plotted; 9000 photons; and 5000 photons.
tion of the continuum and the contribution of photons with energies between 5-6keV to
These figures show the probability distribution for the 1keV portion of the continuum and the contribution of photons with energies between 0-1keV to the data simulation.
The probability distribution on the left represents a continuum of energies between 1keV and 6keV. In the right figure, 16000 random events were recorded according to this distribution.
Stars Simulation with Interferometer Sun with SOH O
3C273 with Chandra Simulation with Interferometer
Fabrication of Interferometer Internal Metrology Four Difficult Areas Hold Mirrors Flat and In Position Formation Flying Hold Detector Craft in Position Pointing Hold Interferometer on Target
Maxim The Black Hole Imager 200 M CONSTELLATION BORESIGHT 10 KM 5000 KM CONVERGER SPACECRAFT COLLECTOR SPACECRAFT (32 PLACES EVENLY SPACED) 0.1µ 10,000cm 2 0.4-7.0keV Effective Area DETECTOR SPACECRAFT
Maxim Pathfinder 100µas Resolution 100cm 2 Effective Area 0.4-2.0keV + 6keV Two Spacecraft Formation Flying at 450km Separation
Maxim Pathfinder Mission Concept 2.5m Optics Spacecraft Carries: - Finder X ray Telescopes Separation 450km 10m 1m 1m Laser Ranging System Size: 2.5x2.5x10m Pitch&Yaw Stability: 3x10-4 arcsec Pitch&Yaw Knowledge: 3x10-5 arcsec Roll Stability: 20 arcsec Position Stability: ----- Carries: Detector Spacecraft Size: Pitch&Yaw Stability: Roll Stability: Lateral Stability: Lateral Knowledge: Focal Stability: X-ray Detector Array Laser Retro Reflectors Precision Thrusters 1x1x1m 20 arcsec 20 arcsec 5mm 50 microns 10 meters
Optics Craft Front View Prime Interferometer Yaw Sensor
Consider, instead, line F. Mount the visible light interferometer on structures at the ends of line F. They then maintain 1nm precision wrt to guide star that lies perpendicular to F. This defines pointing AND maintains lateral position of convergers. (40pm not needed in D and E after all.) A, B, C, D and E all maintain position relative to F.
Detector Energy Resolution Necessary for Fringe Inversi on CC Dis adequate To get large field of view use imaging quantum calorimeter
Metrology Tightest Tolerance is Separation of Entrance Apertures d = λ/20θ for tenth fringe stability At 1keV and 2deg, d=1.7nm At 6keV and 0.5deg, d=1.1nm Requires active thermal control and internal alignment
Laser Beam Split and Collimated Laser Collimator Collimated Beams Cross at 450km Optics Craft 450km to Detector Craft
Detection of Pattern Interference Pattern Interference Pattern Fringes have 14cm period at 450km
Need stability and information wrt to the celestial sphere at level of required resolution. L2 or Fly-away orbit probably necessary Baseline design calls for two stellar interferometers. One each for pitch and yaw SIM class interferometers more than adequate
Delta IV (H) 5m diameter x 19.8m long Baffling Payload Spacecraft Detector Spacecraft (2.2m) 16.4 m Launch Fairing Removed 15.5 m LAUNCH CONFIGURATION Optics Instruments (10m) Optic Spacecraft Systems (2.2m)
Detector Spacecraft ORBIT CONFIGURATION Solar Array (7 m^2, projected area) Optic Spacecraft
DETECTOR SPACECRAFT Payload Fixed Solar Array (6m^2 shown) Stowed Orbit Spacecraft Spacecraft Subsystems are mounted in this volume
200 M CONSTELLATION BORESIGHT Hub Spacecraft Maxim Design 10 KM COLLECTOR SPACECRAFT (32 PLACES EVENLY SPACED) Light from Star CONVERGER SPACECRAFT 5000 KM DELAY LINE SPACECRAFT Hub Craft Converger Craft Delay Craft DETECTOR SPACECRAFT
Full Maxim
Maxim Limitations If pri mary flats are on separate spacecraft then they can be flownfarther apart. Resolution increases. Limited by visible light aspect from stars They re all resolved at 30nano-arcsec! Find non-thermal visible sources Use x-ray interferometry for aspect too. Solve aspect problem and reach 10-9 arcsec
Integrated System Modeling Ball Aerospace Technologies Corporation M. Lieber D. Gallagher Will lead to single most important tool in development and definition of x-ray interferometry
Integrated End-to-End Modeling Environment Integrated modeling seamlessly combines the subsystem models from well established software tools. Allows one to rapidly study parameter interaction of disparate variables from different disciplines. Integrated models facilitate GUI development - muliti-user system tool. Standard interfaces minimizes errors and miscommunications between disciplines ENVIRONMENT INPUTS Thermal Thermal Disturbances Disturbances Mechanical Mechanical Disturbances Disturbances DESIGN PARAMETERS MODELING TOOLS TRASYS/ TRASYS/ SINDA SINDA MATLAB MATLAB Structure Structure Design Design NASTRAN NASTRAN STRUCTURE Control System Control System Design Design Simulink/MATLAB Simulink/MATLAB CONTROLS OPTICS/S ENSOR Optics/Sensor Optics/Sensor Design Design CODE V/ CODE V/ various various SYSTEM MODEL Simulink/MATLAB Optical Errors Optical Errors CODE V CODE V Sensor Sensor Noise Noise MATLAB MATLAB SYSTEM PERFORMANCE VS. SCIENCE METRICS
Example of MAXIM Pathfinder Optical subsystem Optical ray bundle1 [ttt,uuu] u_surf1 RB offsets Out3 Deform map Offsets Sparse array RB offsets Out3 Deform map Offsets1 Sparse array Image plane sav_psf To Workspace2 [ttt,uuu2] u_surf2 Maxim Pathfinder IM Signal processing Wavefront & tilt sensor models [c1] 3 1 In1 2 Telescope mechanism tip/tilt and wavefront control systems Structural dynamics Spacecraft attitude control 1 Optics model Imaging sensor models Image processing Structures, optics, controls, signal processing, disturbances 2 2 1 Ray bundle Optics motion {a1} {a1} {b1} {b1} Sparse reflective mirror1 Sparse reflective mirror2 Sparse reflective mirror3 Sparse reflective mirror4 [c2] [c3] [c4] [c1] [c2] [c3] [c4] 1 Out1
Optical Toolbox: Key Element of Optical Performance Modeling Geometric ray trace Diffraction analysis (PSF outputs) Easy introduction of mirror distortions from thermal or vibration Optics tied to NASTRAN structural model Active control modeling of metrology system and active optics Interfaces with imaging and detection modules Optical ray bundle1 [ttt,uuu] u_surf1 RB offsets Out3 Deform map Offsets [ttt,uuu2] u_surf2 Sparse primary mirror array RB offsets Out3 Deform map Offsets1 Sparse secondary mirror array Image plane sav_psf To Workspace2 See next slide
MAXIM Pathfinder PSFs with Different Number of Optical Elements PSF Image Log image 2 segments 4 segments 32 segments
MAXIM Physical Model Celestrial objects Converger and Delay Line S/C Collectors & Hub S/C Command and Control Detector S/C MAXIM Integrated Model
MAXIM System Modeling Leveraged From NASA and Other Programs GSFC - Expertise and models for formation flying - FF lab Optical metrology - Ball/GSFC Cross Enterprise contract, Ball/JPL Starlight program Integrated modeling environment and MATLAB/Simulink toolset - NGST, TPF, VLT Wavefront control - see next slide
Example Wavefront Control Modeling - Initial Phase Map of NGST Wavefront control tools from NGST program and extensive work on phase retrieval by JPL 10 20 x-decenter y-decenter 30 piston 40 tip 50 tilt 60 10 20 30 40 50 60 10 20 30 40 RMS random segments Random errors for 36 segments = primary [ 1e-4 1e-4 4e-5 1e-5 1e-4 0] 10 x 10-4 8 6 4 [ x-decenter y-decenter piston tip tilt clocking] 50 60 10 20 30 40 50 60 Secondary = offsets -2 02-4 [ 1e-3 1 2 5e-4 3 4 1.5e-5 5-3e-5 6 8e-4 0] [ x-decenter y-decenter piston tip tilt clocking]
Status: X-ray Interferometry in NASA Planning Structure and Evolution of the Universe (SEU) Roadmap Maxim Pathfinder Appears as Mid-Term Mission Candidate Mission for 2008-2013 Maxim Appears as Vision Mission Candidate Mission for >2014 McKee-Taylor Report National Academy Decadal Review of Astronomy Released May 19, 2000 Prominently Recommends Technology Development Money for X-ray Interferometry
X-ray Roadmap to Image a Black Hole Imaging ROSAT Einstein Spectroscopy ASCA RXTE Do they exist? Chandra 100-1000 cm 2 0.5 arc sec XMM Astro-E Optimize MAXIM Parameters Constellation-X 3 m 2 Indirect imaging via spectroscopy 1000 times finer imaging MAXIM Pathfinder 100 cm 2 2 m baseline 100 µarc sec Million times finer imaging MAXIM 1000 cm 2 100-1000 m baseline 100 nas Spectrally Resolved X-ray Where are Conditions in Interferometry Black hole they? the inner disk Demonstration Imager! 2000 2008 2014 2020
Technology Development Start with NIAC and SR&T Funding Mission Specific Funding Maxim Pathfinder New Start 2008 Develop & Test Technology for Maxim MAXIM Five Years after Pathfinder Plan
The Black Hole Disney, 1979 We have already found this black hole and will have these pictures before 2020.